The Solar Optical Telescope
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Solar and Space Physics: a Science for a Technological Society
Solar and Space Physics: A Science for a Technological Society The 2013-2022 Decadal Survey in Solar and Space Physics Space Studies Board ∙ Division on Engineering & Physical Sciences ∙ August 2012 From the interior of the Sun, to the upper atmosphere and near-space environment of Earth, and outwards to a region far beyond Pluto where the Sun’s influence wanes, advances during the past decade in space physics and solar physics have yielded spectacular insights into the phenomena that affect our home in space. This report, the final product of a study requested by NASA and the National Science Foundation, presents a prioritized program of basic and applied research for 2013-2022 that will advance scientific understanding of the Sun, Sun- Earth connections and the origins of “space weather,” and the Sun’s interactions with other bodies in the solar system. The report includes recommendations directed for action by the study sponsors and by other federal agencies—especially NOAA, which is responsible for the day-to-day (“operational”) forecast of space weather. Recent Progress: Significant Advances significant progress in understanding the origin from the Past Decade and evolution of the solar wind; striking advances The disciplines of solar and space physics have made in understanding of both explosive solar flares remarkable advances over the last decade—many and the coronal mass ejections that drive space of which have come from the implementation weather; new imaging methods that permit direct of the program recommended in 2003 Solar observations of the space weather-driven changes and Space Physics Decadal Survey. For example, in the particles and magnetic fields surrounding enabled by advances in scientific understanding Earth; new understanding of the ways that space as well as fruitful interagency partnerships, the storms are fueled by oxygen originating from capabilities of models that predict space weather Earth’s own atmosphere; and the surprising impacts on Earth have made rapid gains over discovery that conditions in near-Earth space the past decade. -
Solar Chromospheric Flares
Solar Chromospheric Flares A proposal for an ISSI International Team Lyndsay Fletcher (Glasgow) and Jana Kasparova (Ondrejov) Summary Solar flares are the most energetic energy release events in the solar system. The majority of energy radiated from a flare is produced in the solar chromosphere, the dynamic interface between the Sun’s photosphere and corona. Despite solar flare radiation having been known for decades to be principally chromospheric in origin, the attention of the community has re- cently been strongly focused on the corona. Progress in understanding chromospheric flare physics and the diagnostic potential of chromospheric observations has stagnated accord- ingly. But simultaneously, motivated by the available chromospheric observations, the ‘stan- dard flare model’, of energy transport by an electron beam from the corona, is coming under scrutiny. With this team we propose to return to the chromosphere for basic understanding. The present confluence of high quality chromospheric flare observations and sophisticated numerical simulation techniques, as well as the prospect of a new generation of missions and telescopes focused on the chromosphere, makes it an excellent time for this endeavour. The international team of experts in the theory and observation of solar chromospheric flares will focus on the question of energy deposition in solar flares. How can multi-wavelength, high spatial, spectral and temporal resolution observations of the flare chromosphere from space- and ground-based observatories be interpreted in the context of detailed modeling of flare radiative transfer and hydrodynamics? With these tools we can pin down the depth in the chromosphere at which flare energy is deposited, its time evolution and the response of the chromosphere to this dramatic event. -
Manual Ls40tha H-Alpha Solar-Telescope
Manual LS40THa H-alpha Solar-Telescope Telescope for solar observation in the H-Alpha wavelength. The H-alpha wavelength is the most impressive way to observe the sun, here prominences at the solar edge become visible, filaments and flares on the surface, and much more. Included Contents: - LS40THa telescope - H-alpha unit with tilt-tuning - Blocking-filter B500, B600, or B1200 - 1.25 inch Helical focuser - Dovetail bar (GP level) for installing at astronomical mounts - 1/4-20 tapped base (standard thread for photo-tripods) inside the dovetail for installing at photo-tripods - Sol-searcher Please note: Please keep the foam insert from the delivery box. The optionally available transport-case for the LS40THa (item number 0554010) is not supplied without such a foam insert, the original foam insert from the delivery box fits exactly into this transport-case. Congratulations and thank you for purchasing the LS40THa telescope from Lunt Solar Systems! The easy handling makes this telescope ideal for starting H-Alpha solar observation. Due to its compact dimensions it is also a good travel telescope for the experienced solar observers. Safety Information: There are inherent dangers when looking at the Sun thru any instrument. Lunt Solar Systems has taken your safety very seriously in the design of our systems. With safety being the highest priority we ask that you read and understand the operation of your telescope or filter system prior to use. Never attempt to disassemble the telescope! Do not use your system if it is in someway compromised due to mishandling or damage. Please contact our customer service with any questions or concerns regarding the safe use of your instrument. -
Formation and Evolution of Coronal Rain Observed by SDO/AIA on February 22, 2012?
A&A 577, A136 (2015) Astronomy DOI: 10.1051/0004-6361/201424101 & c ESO 2015 Astrophysics Formation and evolution of coronal rain observed by SDO/AIA on February 22, 2012? Z. Vashalomidze1;2, V. Kukhianidze2, T. V. Zaqarashvili1;2, R. Oliver3, B. Shergelashvili1;2, G. Ramishvili2, S. Poedts4, and P. De Causmaecker5 1 Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, 8042 Graz, Austria e-mail: [teimuraz.zaqarashvili]@oeaw.ac.at 2 Abastumani Astrophysical Observatory at Ilia State University, Cholokashvili Ave.3/5, Tbilisi, Georgia 3 Departament de Física, Universitat de les Illes Balears, 07122, Palma de Mallorca, Spain 4 Dept. of Mathematics, Centre for Mathematical Plasma Astrophysics, Celestijnenlaan 200B, 3001 Leuven, Belgium 5 Dept. of Computer Science, CODeS & iMinds-iTEC, KU Leuven, KULAK, E. Sabbelaan 53, 8500 Kortrijk, Belgium Received 30 April 2014 / Accepted 25 March 2015 ABSTRACT Context. The formation and dynamics of coronal rain are currently not fully understood. Coronal rain is the fall of cool and dense blobs formed by thermal instability in the solar corona towards the solar surface with acceleration smaller than gravitational free fall. Aims. We aim to study the observational evidence of the formation of coronal rain and to trace the detailed dynamics of individual blobs. Methods. We used time series of the 171 Å and 304 Å spectral lines obtained by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamic Observatory (SDO) above active region AR 11420 on February 22, 2012. Results. Observations show that a coronal loop disappeared in the 171 Å channel and appeared in the 304 Å line more than one hour later, which indicates a rapid cooling of the coronal loop from 1 MK to 0.05 MK. -
Mechanisms of Chromospheric and Coronal Heating a NIXT Solar X-Ray Photo in the Fe XVI Line at 63.5 a Taken on a Rocket Flight on 11 Sept
Mechanisms of Chromospheric and Coronal Heating A NIXT solar X-ray photo in the Fe XVI line at 63.5 A taken on a rocket flight on 11 Sept. 1989 by Leon Golub (see the article on p. 115 of this book) P. Ultnschneider E. R. Priest R. Rosner (Eds.) Mechanisms of Chromospheric and Coronal Heating Proceedings of the International Conference, Heidelberg, 5-8 lune 1990 With 260 Figures Springer-Verlag Berlin Heidelberg GmbH Professor Dr. Peter Ulmschneider Institut für Theoretische Astrophysik. Im Neuenheimer Feld 561. D-69oo Heidelberg. Fed. Rep. ofGermany Professor Dr. Eric R. Priest University of St. Andrews. The Mathematical Institute North Haugh. St. Andrews KY16 9SS. Great Britain Professor Dr. Robert Rosner E. Fermi Institute and Dept. of Astronomy and Astrophysics. 5640 S Ellis Ave .• Chicago. IL 60637. USA Cover picture: In this scenario by Chitre and Davila (see the article on p.402 of this book) acoustic waves shake coronal magnetic loops and get resonantly absorbed in the loop. ISBN 978-3-642-87457-4 ISBN 978-3-642-87455-0 (eBook) DOI 10.I007/978-3-642-87455-0 This work is subject to copyright. All rights are reserved. whether the whole or part of the material is concerned. specifically the rights of translation. reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfilms or in other ways, and storage in data banks. Duplication ofthis publication or parts thereofis only per mitted underthe provisions ofthe German Copyright Law ofSeptember9, 1965. in its current version, and a copy right fee must always be paid. Violations fall under the prosecution act ofthe German Copyright Law. -
Multi-Spacecraft Analysis of the Solar Coronal Plasma
Multi-spacecraft analysis of the solar coronal plasma Von der Fakultät für Elektrotechnik, Informationstechnik, Physik der Technischen Universität Carolo-Wilhelmina zu Braunschweig zur Erlangung des Grades einer Doktorin der Naturwissenschaften (Dr. rer. nat.) genehmigte Dissertation von Iulia Ana Maria Chifu aus Bukarest, Rumänien eingereicht am: 11.02.2015 Disputation am: 07.05.2015 1. Referent: Prof. Dr. Sami K. Solanki 2. Referent: Prof. Dr. Karl-Heinz Glassmeier Druckjahr: 2016 Bibliografische Information der Deutschen Nationalbibliothek Die Deutsche Nationalbibliothek verzeichnet diese Publikation in der Deutschen Nationalbibliografie; detaillierte bibliografische Daten sind im Internet über http://dnb.d-nb.de abrufbar. Dissertation an der Technischen Universität Braunschweig, Fakultät für Elektrotechnik, Informationstechnik, Physik ISBN uni-edition GmbH 2016 http://www.uni-edition.de © Iulia Ana Maria Chifu This work is distributed under a Creative Commons Attribution 3.0 License Printed in Germany Vorveröffentlichung der Dissertation Teilergebnisse aus dieser Arbeit wurden mit Genehmigung der Fakultät für Elektrotech- nik, Informationstechnik, Physik, vertreten durch den Mentor der Arbeit, in folgenden Beiträgen vorab veröffentlicht: Publikationen • Mierla, M., Chifu, I., Inhester, B., Rodriguez, L., Zhukov, A., 2011, Low polarised emission from the core of coronal mass ejections, Astronomy and Astrophysics, 530, L1 • Chifu, I., Inhester, B., Mierla, M., Chifu, V., Wiegelmann, T., 2012, First 4D Recon- struction of an Eruptive Prominence -
Can You Spot the Sunspots?
Spot the Sunspots Can you spot the sunspots? Description Use binoculars or a telescope to identify and track sunspots. You’ll need a bright sunny day. Age Level: 10 and up Materials • two sheets of bright • Do not use binoculars whose white paper larger, objective lenses are 50 • a book mm or wider in diameter. • tape • Binoculars are usually described • binoculars or a telescope by numbers like 7 x 35; the larger • tripod number is the diameter in mm of • pencil the objective lenses. • piece of cardboard, • Some binoculars cannot be easily roughly 30 cm x 30 cm attached to a tripod. • scissors • You might need to use rubber • thick piece of paper, roughly bands or tape to safely hold the 10 cm x 10 cm (optional) binoculars on the tripod. • rubber bands (optional) Time Safety Preparation: 5 minutes Do not look directly at the sun with your eyes, Activity: 15 minutes through binoculars, or through a telescope! Do not Cleanup: 5 minutes leave binoculars or a telescope unattended, since the optics can be damaged by too much Sun exposure. 1 If you’re using binoculars, cover one of the objective (larger) lenses with either a lens cap or thick piece of folded paper (use tape, attached to the body of the binoculars, to hold the paper in position). If using a telescope, cover the finderscope the same way. This ensures that only a single image of the Sun is created. Next, tape one piece of paper to a book to make a stiff writing surface. If using binoculars, trace both of the larger, objective lenses in the middle of the piece of cardboard. -
Ground-Based Solar Physics in the Era of Space Astronomy a White Paper Submitted to the 2012 Heliophysics Decadal Survey
Ground-Based Solar Physics in the Era of Space Astronomy A White Paper Submitted to the 2012 Heliophysics Decadal Survey T. Ayres1, D. Longcope2 (on behalf of the 2009 AURA Solar Decadal Committee) Chromosphere-Corona at eclipse Hα filtergram Photospheric spots & bright points Same area in chromospheric Ca+ 1Center for Astrophysics and Space Astronomy, 389 UCB, University of Colorado, Boulder, CO 80309; [email protected] (corresponding author) 2Montana State University SUMMARY. A report, previously commissioned by AURA to support advocacy efforts in advance of the Astro2010 Decadal Survey, reached a series of conclusions concerning the future of ground-based solar physics that are relevant to the counterpart Heliophysics Survey. The main findings: (1) The Advanced Technology Solar Telescope (ATST) will continue U.S. leadership in large aperture, high-resolution ground-based solar observations, and will be a unique and powerful complement to space-borne solar instruments; (2) Full-Sun measurements by existing synoptic facilities, and new initiatives such as the Coronal Solar Magnetism Observatory (COSMO) and the Frequency Agile Solar Radiotelescope (FASR), will balance the narrow field of view captured by ATST, and are essential for the study of transient phenomena; (3) Sustaining, and further developing, synoptic observations is vital as well to helioseismology, solar cycle studies, and Space Weather prediction; (4) Support of advanced instrumentation and seeing compensation techniques for the ATST, and other solar telescopes, is necessary to keep ground-based solar physics at the cutting edge; and (5) Effective planning for ground-based facilities requires consideration of the synergies achieved by coordination with space-based observatories. -
Astronomy Astrophysics
A&A 424, 289–300 (2004) Astronomy DOI: 10.1051/0004-6361:20040403 & c ESO 2004 Astrophysics Dynamics of solar coronal loops II. Catastrophic cooling and high-speed downflows D. A. N. Müller1,2, H. Peter1, and V. H. Hansteen2 1 Kiepenheuer-Institut für Sonnenphysik, Schöneckstr. 6, 79104 Freiburg, Germany e-mail: [email protected];[email protected] 2 Institute of Theoretical Astrophysics, University of Oslo, PO Box 1029, Blindern 0315, Oslo, Norway e-mail: [email protected] Received 7 March 2004 / Accepted 14 May 2004 Abstract. This work addresses the problem of plasma condensation and “catastrophic cooling” in solar coronal loops. We have carried out numerical calculations of coronal loops and find several classes of time-dependent solutions (static, periodic, irregular), depending on the spatial distribution of a temporally constant energy deposition in the loop. Dynamic loops exhibit recurrent plasma condensations, accompanied by high-speed downflows and transient brightenings of transition region lines, in good agreement with features observed with TRACE. Furthermore, these results also offer an explanation for the recent EIT observations of De Groof et al. (2004) of moving bright blobs in large coronal loops. In contrast to earlier models, we suggest that the process of catastrophic cooling is not initiated by a drastic decrease of the total loop heating but rather results from a loss of equilibrium at the loop apex as a natural consequence of heating concentrated at the footpoints of the loop, but constant in time. Key words. Sun: corona – Sun: transition region – Sun: UV radiation 1. Introduction observations, compatible with “dramatic evacuation” of active region loops triggered by rapid, radiation dominated cooling. -
Arxiv:1708.06781V1 [Astro-Ph.SR] 22 Aug 2017 Very Complex Region That Is Difficult to Directly Diagnose
Draft version August 24, 2017 Preprint typeset using LATEX style emulateapj v. 12/16/11 TWO-DIMENSIONAL RADIATIVE MAGNETOHYDRODYNAMIC SIMULATIONS OF PARTIAL IONIZATION IN THE CHROMOSPHERE. II. DYNAMICS AND ENERGETICS OF THE LOW SOLAR ATMOSPHERE Juan Mart´ınez-Sykora1,2, Bart De Pontieu2,3, Mats Carlsson3, Viggo H. Hansteen3,2, Daniel Nobrega-Siverio´ 4,5, and Boris V. Gudiksen3 1 Bay Area Environmental Research Institute, Petaluma, CA 94952, USA 2 Lockheed Martin Solar and Astrophysics Laboratory, Palo Alto, CA 94304, USA 3 Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029 Blindern, N-0315 Oslo, Norway 4 Instituto de Astrof´ısicade Canarias, 38200 La Laguna (Tenerife), Spain and 5 Department of Astrophysics, Universidad de La Laguna, E-38200 La Laguna (Tenerife), Spain Draft version August 24, 2017 ABSTRACT We investigate the effects of interactions between ions and neutrals on the chromosphere and over- lying corona using 2.5D radiative MHD simulations with the Bifrost code. We have extended the code capabilities implementing ion-neutral interaction effects using the Generalized Ohm's Law, i.e., we include the Hall term and the ambipolar diffusion (Pedersen dissipation) in the induction equation. Our models span from the upper convection zone to the corona, with the photosphere, chromosphere and transition region partially ionized. Our simulations reveal that the interactions between ionized particles and neutral particles have important consequences for the magneto-thermodynamics of these modeled layers: 1) ambipolar diffusion increases the temperature in the chromosphere; 2) sporadically the horizontal magnetic field in the photosphere is diffused into the chromosphere due to the large ambipolar diffusion; 3) ambipolar diffusion concentrates electrical currents leading to more violent jets and reconnection processes, resulting in 3a) the formation of longer and faster spicules, 3b) heating of plasma during the spicule evolution, and 3c) decoupling of the plasma and magnetic field in spicules. -
IRIS-4 Abstracts
IRIS-4 Abstracts List of Presenters Invited Talks Tutorials Paul Boerner Joel Allred & Adam Kowalski Mats Carlsson Mats Carlsson & Jorrit Leenaarts Lindsay Fletcher Boris Gudiksen & Juan Martinez-Sykora Joten Okamoto Tiago Pereira Luc Rouppe van der Voort Paola Testa Contributed Talks Posters Markus Aschwanden Eugene Avrett Stephen Bradshaw Jeffrey Brosius Sean Brannon Lakshmi Pradeep Chitta Nai-Hwa Chen Bart De Pontieu Mark Cheung Fernando Delgado Steven Cranmer Malcolm Druett Brian Fayock Haihong Che Thomas Golding Catherine Fischer David Graham Bernhard Fleck Lijia Guo Petr Heinzel Petr Heinzel Sarah Jaeggli Phil Judge Jayant Joshi Charles Kankelborg Ryuichi Kanoh Yukio Katsukawa Tomoko Kawate Graham Kerr Yeon-Han Kim Sasha Kosovichev Irina Kitiashvili Kyong Sun Lee Shunya Kono Peter Levens Adam F. Kowalski Ying Li Terry Kucera Hsiao-Hsuan Lin David Kuridze Wei Liu Hannah Kwak Wenjuan Liu Scott McIntosh Juan Martinez-Sykora Sargam Mulay Tiago Pereira Joten Okamoto Vanessa Polito Bala Poduval Fatima Rubio da Costa Daniel Price Donald Schmit Bhavna Rathore Hui Tian Luc Rouppe van der Voort Jean-Claude Vial Danny Ryan Gregal Vissers Jamie Ryan Sven Wedemeyer-Boehm Martin Snow Jean-Pierre Wuelser Ted Tarbell Vasyl Yurchyshyn Akiko Tei Hui Tian Sven Wedemeyer-Boehm Lauren Woolsey Jean-Pierre Wuelser Matthew West List of Presenters Page 1 Invited Talks Planning coordinated observations with IRIS Paul Boerner, Lockheed Martin Solar and Astrophysics Laboratory Much of the power of IRIS comes from the flexibility of its operating modes, which enable observers to optimize the cadence, spatial and spectral coverage and resolution for a particular science target and coordination. In this talk, we present a practical overview of how best to make these choices in consultation with the IRIS science team in order to ensure successful coordinated observations. -
A Recommendation for a Complete Open Source Policy
A recommendation for a complete open source policy. Authors Steven D. Christe, Research Astrophysicist, NASA Goddard Space Flight Center, SunPy Founder and Board member Jack Ireland, Senior Scientist, ADNET Systems, Inc. / NASA Goddard Space Flight Center, SunPy Board Member Daniel Ryan, NASA Postdoctoral Fellow, NASA Goddard Space Flight Center, SunPy Contributor Supporters SunPy Board ● Monica G. Bobra, Research Scientist, W. W. Hansen Experimental Physics Laboratory, Stanford University ● Russell Hewett, Research Scientist, Unaffiliated ● Stuart Mumford, Research Fellow, The University of Sheffield, SunPy Lead Developer ● David Pérez-Suárez, Senior Research Software Developer, University College London ● Kevin Reardon, Research Scientist, National Solar Observatory ● Sabrina Savage, Research Astrophysicist, NASA Marshall Space Flight Center ● Albert Shih, Research Astrophysicist, NASA Goddard Space Flight Center Joel Allred, Research Astrophysicist, NASA Goddard Space Flight Center Tiago M. D. Pereira, Researcher, Institute of Theoretical Astrophysics, University of Oslo Hakan Önel, Postdoctoral researcher, Leibniz Institute for Astrophysics Potsdam, Germany Michael S. F. Kirk, Research Scientist, Catholic University of America / NASA GSFC The data that drives scientific advances continues to grow ever more complex and varied. Improvements in sensor technology, combined with the availability of inexpensive storage, have led to rapid increases in the amount of data available to scientists in almost every discipline. Solar physics is no exception to this trend. For example, NASAʼs Solar Dynamics Observatory (SDO) spacecraft, launched in February 2010, produces over 1TB of data per day. However, this data volume will soon be eclipsed by new instruments and telescopes such as the Daniel K. Inouye Solar Telescope (DKIST) or the Large Synoptic Survey Telescope (LSST), which are slated to begin taking data in 2020 and 2022, respectively.